Figure REF  shows the probability distribution functions
(PDFs) of the specific star formation rate (sSFR), color
(as indicated by \((g-r)^{0.1}\) ), \(D_n4000\) 
and \(\sigma _{*}\)  separately for AGN host galaxies,
star-forming and quiescent galaxies, in four stellar mass bins.
Here results are shown for cAGN (central AGNs) and the two
control samples, cSF\(^{\rm c}\)  and cQ\(^{\rm c}\) , as defined in
Section REF . By definition, quiescent galaxies have
lower sSFR than star-forming galaxies, and the two populations
have almost no overlap in their sSFR distributions within individual
stellar mass bins. Because of the strong correlation of sSFR with
color and \(D_n4000\) , quiescent galaxies have higher \((g-r)^{0.1}\) 
and \(D_n4000\)  than star-forming galaxies. Quiescent galaxies
also have larger \(\sigma _{*}\)  than star-forming galaxies of the
same stellar mass, consistent with the fact that the fraction of
quiescent galaxies increases rapidly with \(\sigma _{*}\) 
[1]}, [2]}. In addition, the color and \(D_n4000\) 
for both populations increase gradually with stellar mass,
because galaxies of lower masses in general are younger and metal
poorer.
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